Adiabatic stability of toroidal magnetic fields in differentially rotating stars

Details Adiabatic stability of toroidal magnetic fields in differentially rotating stars Adiabatic stability of toroidal magnetic fields in differentially rotating stars

Jun 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979mnras.187..769c&link_type=abstract

Monthly Notices of the Royal Astronomical Society, vol. 187, June 1979, p. 769-776. Research supported by the Science Research

Astronomy and Astrophysics

Astronomy

21

Adiabatic Conditions, Magnetohydrodynamic Stability, Stellar Magnetic Fields, Stellar Rotation, Potential Energy, Small Perturbation Flow, Stellar Models, Stellar Temperature

Scientific paper

The adiabatic stability with respect to axisymmetric perturbations of a toroidal magnetic field in a differentially rotating star in which the magnetic and rotation axes coincide is examined. It has been suggested that magnetic fields in rotating stars could undergo local MHD instabilities in cooling degenerate stars; it has also been hypothesized that in solar-type stars, differential rotation could create a strong toroidal field in the core by winding up a weak poloidal field. Sufficient conditions for magnetic stability are derived through use of methods developed by Frieman and Rotenburg (1960) and Lynden-Bell and Ostriker (1967).

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